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At least 307 records · Page 17
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NASA NTRS1977

Isotopic and chemical investigations on Angra dos Reis

Isotope ratios and chemical abundance measurements for a variety of elements are reported for total meteorite and mineral separates of the Angra dos Reis achondrite. U-Pb, Th-Pb, and Pb-Pb ages are concordant at 4.54 eons for the total meteorite and for high-purity whitlockite, which indicates that Angra dos Reis is an early planetary differentiate that has not been disturbed for these systems since 4.54 eons ago. The implications of different ratios of Sr-87 and Sr-86 found in different components are discussed. Xe isotopic measurements show that Pu-244 was enriched in the whitlockite relative to the pyroxene by a factor of about 18. Chemical enrichment factors between the whitlockite and the fassaitic pyroxene in Angra dos Reis are presented

Wasserburg, G. J.↗
NASA NTRS1977

The Kramer Creek, Colorado meteorite - A new L4 chondrite

Results of bulk chemical analyses and mineralogical and petrographic studies of a chondrite found at Kramer Creek, Colorado, are reported. The meteorite has been classified as an L-group chondrite on the basis of its bulk chemistry, the fayalite content of its olivine (21.7%) and the ferrosilicate content of its pyroxene (18.3%). The presence of interstitial glass and the iron oxide percent mean deviations for olivine and low-Ca pyroxene (2.4 and 4.6%) place the specimen in petrologic group 4 of the Van Schmus and Wood classification (1967)

Gibson, E. K., Jr.↗
NASA NTRS1978

Are the stratospheric dust particles meteor ablation debris or interplanetary dust?

Natural and laboratory created fusion crusts and debris from artificial meteor samples were used to develop criteria for recognizing meteor ablation debris in a collection of 5 to 50 micron particles from the stratosphere. These laboratory studies indicate that meteor ablation debris from nickel-iron meteoroids produce spherules containing taenite, wuestite, magnetite, and hematite. These same studies also indicate that ablation debris from chondritic meteoroids produce spheres and fragmentary debris. The spheres may be either silicate rich, containing zoned olivine, magnetite, and glass, or sulfide rich, containing iron oxides (e.g., magnetite, wuestite) and iron sulfides (e.g., pyrrhotite, pentlandite). The fragmentary debris may be either fine-grained aggregates of olivine, magnetite, pyroxene, and occasionally pyrrhotite (derived from the meteorite matrix) or individual olivine and pyroxene grains (derived from meteorite inclusions).

Blanchard, M. B.↗
NASA NTRS1978

The Inman, McPherson County, Kansas meteorite

The Inman meteorite (find, 1966) is a single relatively unweathered stone of 7.25 kg that contains fresh metal and only a few weathering products away from fractures. It has a pronounced chondritic texture, with 38 vol% of the meteorite being made up of chondrules of virtually all textural types. The recalculated bulk analysis, in particular ratios involving iron content, indicate that Inman is an L-group chondrite. The pronounced chondritic texture; the compositional variation of olivine, pyroxene, chromite, and ilmenite; and the presence of a fine-grained nearly opaque matrix, glass, and twinned monoclinic low-Ca pyroxene indicate that the chondrite belongs to petrologic type 3.

Keil, K.↗
NASA NTRS1977

Temperature dependence of Fe/++/ crystal field spectra - Implications to mineralogical mapping of planetary surfaces

Results are reported of Fe(++) crystal field spectral measurements for olivines and pyroxenes up to 400 C. The results are correlated with crystal structure data at elevated temperatures, and the validity of remote-sensed identifications of minerals on hot surfaces of the moon and Mercury is assessed. Two techniques were used to obtain spectra of minerals at elevated temperatures using a spectrophotometer. One employed a diamond cell assembly or a specially designed sample holder to measure polarized absorption spectra of heated single crystals. For the other technique, a sample holder was designed to attach to a diffuse reflectance accessory to produce reflectance spectra of heated powdered samples. Polarized absorption spectra of forsterite at 20-400 C are shown in a graph. Other graphs show the temperature dependence of Fe(++) crystal field bands in olivines, the diffuse reflectance spectra of olivine at 40-400 C, the polarization absorption spectra of orthopyroxene at 30-400 C, the diffuse reflectance spectra of pigeonite at 40-400 C, and unpolarized absorption spectra of lunar pyroxene from Apollo 15 rock 15058.

Sung, C.-M.↗
NASA NTRS1977

Lead isotope studies of mare basalt 70017

Uranium, thorium, and isotopic lead data for components of basalt 70017 are reported, and it is found that the whole rock, pyroxene, and ilmenite points in a concordia diagram plot along a chord intersecting the curve at 3.7 and 4.33 eons. The plagioclase data do not seem to lie on this line. The data for 70017 appear to plot along a distinctly different chord in a concordia diagram than do the data for 75055 and 75035, two other Apollo 17 mare basalts. The lead data are in accord with Sm-Nd results. A 3.7 eon crystallization age for 70017 would be consistent with the same kind of parentless lead that is indicated by previous studies of soils and soil breccias from stations at Taurus-Littrow. The Th/U ratio in ilmenite is 2.2, and the concentrations of these two elements are approximately twice those in pyroxene.

Mattinson, J. M.↗
NASA NTRS1977

Slowly cooled microgabbros 15555 and 15065

An experimental study involving equilibration of Apollo 15 samples 15555 and 15065 in high-purity iron capsules is described. Comparison of mineral zoning trends with the experimental sequence suggests that the early crystallizing phases in the rock maintained surface equilibrium with the liquid. Olivine and pyroxene chemistry indicates that 15555 cooled slightly more rapidly than 15065, which cooled at approximately 0.2-0.3 C/day. It is suggested that 15065 and 15555 represent liquid compositions, and that these liquids appear to have been fractionated during ascent through the crust (15065), or to have been derived from an olivine-pyroxene source (15555) with Fe/(Fe + Mg) approximately equal to 0.73 at a depth between 150-200 km.

Walker, D.↗
NASA NTRS1975

Petrologic evidence for a plutonic igneous origin of anorthositic norite clasts in 67955 and 77017

Clasts of anorthositic norite in 67955 and 77017, and several other samples, are suggested to represent material which crystallized from a silicate magma in a plutonic environment. Although no statement can be made regarding the ultimate origin of the parent melt, its composition was relatively felsic, starting within the primary field of crystallization of either plagioclase or spinel. The sequence of crystallization was: plagioclase (and/or spinel) olivine - low-Ca pyroxene - high-Ca pyroxene.

Ashwal, L. D.↗
NASA NTRS1978

Luna 24: 90-150 micrometer fraction - Implications for remote sampling of regolith

An analysis of the mineral grains and glasses found in the 90 to 150 micron fraction of the Luna 24 core sample is presented and implications for the automatic collection of planetary and asteroidal regoliths are discussed. Electron microprobe analysis for pyroxene, olivine, plagioclase, opaque minerals and glass in samples at various depths indicate that polymineralic grains have compositions similar to those of gabbroic and basaltic fragments from coarser samples, while monomineralic grains contain an additional population of Mg-rich olivines and pyroxene. Most of the glasses are found to be related to mare basalts or local regolith, with nonmare material represented by glasses of highland basalt and low K Fra Mauro composition. It is concluded that as regards mineralogy and petrology, a single grab sample would have been as useful and a series of grab samples on a long traverse would have been more useful than the Luna 24 core sample, with the fine sample being more informative than the coarse.

Papp, H. A.↗
NASA NTRS1978

Chemistry and petrology of Luna 24 lithic fragments and less than 250-micron soils - Constraints on the origin of VLT mare basalts

Results are reported on a combined INAA-petrologic study of 17 small (0.2-1.5 mg) Luna 24 lithic and mineral fragments and INAA study of 5 bulk soils and mineral separates from gabbro 24170. Lithic and mineral fragments are classified into VLT mare basalts (ferrobasalt and metabasalts), low-Ti, variolitic mare basalt, gabbros, melt rock and soil breccia. Data indicate 5 possible magma types, represented by: (1) VLT ferrobasalt and gabbro fragments, with low-TiO2 (about 1%), slightly bow-shaped REE pattern, and low REE concentrations (5-10X chondritic); (2) a ferrobasalt (Laul et al., 1978) and metabasalt fragments with major and trace element contents similar to (1), but positive Eu anomalies; (3) one gabbro fragment with distinctive pyroxene compositional trend (increasing Ti with nearly constant Fe/Fe + Mg) and highest REE contents of any Luna 24 mare basaltic sample, (4) a gabbro fragment with considerably less V and Cr2O3 than ferrobasalt and metabasalt fragments; and (5) variolitic basalt fragment with higher Ti2(2.3%) than other Luna 24 basalts and pyroxene that has increasing then decreasing Ti with increasing Fe/Fe + Mg. Trace element data place constraints on the nature of the source region and possible parent magmas for the Luna 24 VLT ferrobasalt.

Ma, M.-S.↗
NASA NTRS1978

Genesis of Apollo 15 olivine normative mare basalts - Trace element correlations

Chemical and petrographic studies of 21 Apollo 15 rake basalts are reported; one pyroxene-phyric basalt, four olivine-phyric basalts, 15 olivine microgabbros, and one brecciated basalt are distinguished. The olivine-normative basalts (i.e., all samples but the pyroxene-phyric basalt) show correlation trends of La/Sm vs. La and Sm/Eu vs. La that are within the observed dispersion ranges of La/Sm and Sm/Eu ratios for a single lava flow. Trace element fractionation trends in the sample could be due to mobilization (perhaps by filter pressing) of fractionated residual liquid during the crystallization of a lava flow. However, it is also possible that the suite of olivine-normative basalts represents several basalt flows produced by partial melting of cumulate layers having interstitial liquids with variable trace-element compositions.

Ma, M.-S.↗
NASA NTRS1978

Clast assemblages of possible deep-seated /77517/ and immiscible-melt /77538/ origins in Apollo 17 breccias

Breccia samples 77517 and 77538 are composed of abundant mineral and lithic clasts set in porous, poorly sintered matrices. Clast assemblages in the two rocks are of contrasting composition and origin. Breccia 77517 has Mg-rich olivine and pyroxene and calcic plagioclase clasts, indicating limited, almost exclusively ANT-suite parentage. A significant feature is the presence of an assemblage (aluminous enstatite, forsterite, anorthite, aluminous spinel) corresponding to spinel cataclasite, a rock type of deep-seated (about 60 km) crustal origin. Breccia 77538 contains Fe-rich pyroxene and rather sodic plagioclase clasts, indicative of predominantly KREEP and/or mare derivation. An important feature is the occurrence of high-K and high-Fe lithic clasts whose compositions resemble those of immiscible-melts produced during late-stage magmatic crystallization, and which probably originated via silicate liquid immiscibility in a KREEP or mare basalt magma. Both rocks contain numerous fine-grained breccia clasts which represent material that has been modified by impact processes at or very near the moon's surface.

Warner, R. D.↗
NASA NTRS1978

Mineralogy, textures and mode of formation of a hibonite-bearing Allende inclusion

The origin of a Type A, hibonite-rich, coarse-grained inclusion is investigated with the electron microprobe and petrographic and scanning electron microscopes. The primary phases are hibonite, rhonite, Ti-Al-pyroxene, spinel, perovskite and melilite. Evidence for the crystallization of the bulk of the primary phases, hibonite and melilite, from a melt is lacking, suggesting that they may have condensed directly from a solar nebular gas instead. Primary phases were intensely altered during a later condensation event which deposited grossular, anorthite, nepheline and wollastonite in veins and cavities. Four or five condensate rims were deposited as successive layers on the outside of the inclusion. From inside to outside, they consist of perovskite + spinel, nepheline + anorthite, Ti-Al-pyroxene + diopside, hedenbergite + or - wollastonite + or - andradite and, finally, prisms of diopside and hedenbergite with wollastonite and andradite. Reverse zoning in melilite; alteration phases and rim phases, which are not stable condensates from a gas of solar composition; and details of the sequence of rim condensates all suggest that the entire condensation history of this inclusion was interrupted by changes in pressure and/or temperature and/or gas phase composition.

Allen, J. M.↗
NASA NTRS1979

Remnants from the ancient lunar crust - Clasts from consortium breccia 73255

The paper examines analyses of clasts from consortium breccia 73255. It was shown that the basalts are high-alumina, and contain low, unfractionated abundances; the felsite is similar in major element composition and relative REE abundances to the felsites from 73215 and 12013; and the ANT materials are similar to the ANT clasts in other Apollo 17 breccias. Model calculations show that the pyroxene anorhosite has equilibrated with a very evolved liquid, and it is indicated that there was once a liquid with an evolved REE composition which was the parent of the pyroxene anorthosite.

Blanchard, D. P.↗
NASA NTRS1979

Li, Be, and B in minerals of a refractory-rich Allende inclusion

The abundances of Li, Be, and B and the isotopic ratios of Li and B have been measured by ion microprobe in melilite, pyroxene, anorthite, and spinel grains in a coarse-grained inclusion from the Allende meteorite. Based on the measurements, it is estimated that the bulk inclusion contains 200 ppb Li, 310 ppb Be, and 18 ppm B. The B is probably due to contamination. The Li-7/Li-6 ratios in spinels, pyroxene, and melilite are indistinguishable at the + or - 15% level and lie within the uncertainty (+ or - 15%) of the range of values reported for samples of the earth and meteorites. It has been determined that this inclusion contains an excess of Al-correlated Mg-26, implying that Al-26 was once present in it. The Li-Be-B effects for two solar-system proton-irradiation models which propose to account for Al-26 in Allende inclusions have been calculated. It is found that the predicted Li-Be-B abundances and isotopic ratios are grossly different from those observed in any solar-system materials.

Phinney, D.↗
NASA NTRS1979

Vacuum ultraviolet reflectance spectra of group H chondrites

The spectral reflectances of seventeen group H chondrites have been measured in the vacuum ultraviolet region, from 5 to 14 eV photon energy (250 to 90 nm, wavelength), as part of a survey of all meteorite types. Olivines, ortho-, and clino- pyroxenes are the three most important silicate minerals in these meteorites, and the spectrum of each mineral contains a distinct peak caused by a transition believed to be excitonic in nature and involving the valence-conduction bandgap. The energy at which this peak occurs varies as a function of mineral composition, and this variation has been determined from the spectra of a number of mineral standards. The observed positions of the olivine and pyroxene peaks in the meteorite spectra are compared to predicted positions based on the standard minerals.

Wagner, J. K.↗
NASA NTRS1979

Complex igneous processes and the formation of the primitive lunar crustal rocks

Crystallization of a magma ocean with initial chondritic Ca/Al and REE ratios such as proposed by Taylor and Bence (TB, 1975), is capable of producing the suite of primitive crustal rocks if the magma ocean underwent locally extensive assimilation and mixing in its upper layers as preliminary steps in formation of an anorthositic crust. Lunar anorthosites were the earliest permanent crustal rocks to form the result of multiple cycles of suspension and assimilation of plagioclase in liquids fractionating olivine and pyroxene. There may be two series of Mg-rich cumulate rocks: one which developed as a result of the equilibration of anorthositic crust with the magma ocean; the other which formed in the later stages of the magma ocean during an epoch of magma mixing and ilmenite crystallization. This second series may be related to KREEP genesis. It is noted that crystallization of the magma ocean had two components: a low pressure component which produced a highly fractionated and heterogeneous crust growing downward and a high pressure component which filled in the ocean from the bottom up, mostly with olivine and low-Ca pyroxene.

Longhi, J.↗
NASA NTRS1980

Spectroscopic evidence for two achondrite parent bodies - Asteroids 349 Dembowska and 4 Vesta

A Fourier spectrometer was used to obtain IR spectra of asteroids 349 Dembowska and 4 Vesta. The spectrum of Dembowska shows olivine and pyroxene with an olivine/pyroxene abundance ratio greater than 2, and possibly as high as 10. This is probably an unsampled achondritic composition, similar to the unique achondrite ALHA 77005. Dembowska's mineralogy therefore appears related to the achondrites; pyroxene and plagioclase feldspar are seen, with a pyroxene/feldspar abundance ratio between 1.5 and 2.0. Time-resolved observations over one-half of the rotation period indicate compositional homogeneity; both 349 Dembowska and 4 Vesta can be considered as candidates for the parent bodies of igneous meteorites.

Feierberg, M. A.↗